摘要
扼要地介绍了色球和日冕加热问题的研究历史。随着空间太阳观测技术的进步，人们认识到色球和日冕加热机制主要与MHD过程有关。因此，在本文中着重介绍四种MHD色球和日冕加热机制：（1）阿尔芬波；（2）MHD湍动；（3）场向电流；（4）磁重联。由于这四种加热机制的有效性都需要通过高分辨率观测来判定，所以空间太阳观测对于研究色球和日冕加热问题具有重大意义。
The history of researches on the chromospheric and coronal heating is introduced briefly in this article. With the continuous progresse of space solar observations, it has been revealed that solar magnetic fields pny very importat roles in the heating. Here we discuss four mechanisms concerning Alfven waves, MHD turbulences, field-aligned currnts and magnetic field line recon nections. Since the availability of these mechedsms should be tested through high sensitive solar observations, advanced space solar observations are very important for future researches.
出处
《天文学进展》
CSCD
北大核心
1996年第3期304-311,共8页
Progress In Astronomy
